Second version of this maps pager implemented a fix to the noise level: 2017-01-19
This is the third version. It has been updated to use ℓmax = 1024. Also added unlensed-ΛCDM maps and combined maps with four different levels of AL.
See the CMB-S4 wiki for a description of the instrumental and astrophysical specification for Data Challenge 1.
The pager below lets you inspect T, Q, and U maps for the first five realizations (out of 100).
T maps are plotted with color scale ±250 μK; Q and U maps are plotted with color scale ±10 μK.
Types of simulated maps are:
Mask — Noise inverse variance
Combined — Noise + ΛCDM + Gaussian dust + Gaussian sync. The ΛCDM component contains lensing signal corresponding to AL = 0.03, 0.1, 0.3, or 1.
Dust — Gaussian dust only
Sync — Gaussian synchrotron only
LCDM — Lensed-ΛCDM only
Noise — Noise only
Some observations (sanity check) from these plots:
The T map is dominated by CMB temperature fluctuations at all frequencies. Noise is visible only in the outermost ring of pixels, where the inverse variance map falls to zero. At 30 and 40 GHz, the large beam size (76.6, 57.5 arcmin) noticeably smooths out the temperature anisotropy. If you select dust or sync, the foregrounds can just barely be seen at the highest / lowest frequency with this ±250 μK color scale.
The Q and U maps show the CMB E-mode signal in the intermediate frequencies (85–155 GHz). At 30–40 GHz, we see the synchrotron signal. At 220 and especially 270 GHz, the dust signal begins to dominate, with power at larger angular scales and less preference for E modes.
If you flip between “combined, AL=0.03” and “combined, AL=1.0“, you can see the signal shift subtly.